Type of variability: EA

Algol (Beta Persei)-type eclipsing systems.

Binaries with spherical or slightly ellipsoidal components. It is possible to specify, for their light curves, the moments of the beginning and end of the eclipses. Between eclipses the light remains almost constant or varies insignificantly because of reflection effects, slight ellipsoidality of components, or physical variations. Secondary minima may be absent. An extremely wide range of periods is observed, from 0.2 to >= 10000 days. Light amplitudes are also quite different and may reach several magnitudes.

General Catalog of Variable Stars

4842

stars

0

observed in last month


Name Type Brightness
HR AND EA 14.7 – 15.4
HS AND EA 12.7 – 14.1
IL AND EA 15.7 – 17.0
IP AND EA 16.8 – 17.3
KN AND EA 11.7 – 13.1
KP AND EA 11.5 – 12.9
LW AND EA 15.5 – 16.4
MM AND EA 16.5 – 17.8
MO AND EA 13.2 – 16.1
NP AND EA 15.29 – 16.1
NZ AND EA 14.9 – 16.3
OT AND EA 7.32 – 7.7
PP AND EA 14.3 – 16.6
QR AND EA 12.16 – 13.0
RT AND EA 8.97 – 9.8
SY AND EA 10.7 – 12.2
TT AND EA 11.5 – 13.1
TW AND EA 8.98 – 11.0
UU AND EA 11.2 – 14.2
V0342 AND EA 7.58 – 7.7